Clarifying these outstanding issues will allow us to identify which combinations of theoretical supernova yield models, \(y_{SN,i}\) , provide the best fit to the observations of the ICM and IGrM (avoiding regions affected by dust depletion if applicable), offering important clues about open aspects of stellar astrophysics. For instance, it was realized very early on that abundance ratios measured from X-ray spectra of the ICM could be used to distinguish between various SNIa explosion mechanisms, preferring a deflagration over a delayed detonation model [1]}. Similar conclusions were tentatively reached for the IGrM [2]}, [3]}. It is becoming clear, however, that both an improvement in the data quality and increased accuracy in the yield models are necessary before robust conclusions can be drawn ([4]}, [5]}, [6]}, [7]}; for a review, see [8]}). Significant progress is expected to be driven in this sense by upcoming high-resolution X-ray spectroscopy studies.
